Fall 2023 Joint Meeting of the Texas Section of the APS, Texas Section of the AAPT & Zone 13 of the SPS
Thursday–Saturday, October 12–14, 2023;
Angelo State University, San Angelo, Texas
Session F06: SPS
1:00 PM–2:12 PM,
Friday, October 13, 2023
Angelo State University
Room: VIN 146
Chair: Scott Williams, Angelo State University
Abstract: F06.00004 : Skyrme and surface parameters influence on accretion disks in neutron star crusts
1:36 PM–1:48 PM
Abstract
Presenter:
Carlos Davila
(Dallas college)
Authors:
Carlos Davila
(Dallas college)
William G Newton
(Texas A&M University–Commerce)
Neutron stars are incredibly compact celestial objects primarily formed of neutrons, resulting from the collapse of a super massive star. These stars often exist in binary systems with other stars, and a specific subtype known as Low-Mass X-ray Binary (LMXB) neutron stars pairs with low-mass stars. In these systems, the neutron star orbits closely enough to siphon matter from its companion, creating an accretion disk around itself. This environment is crucial for studying extreme physical conditions, such as strong gravity, high magnetic fields, and matter at extreme densities, helping us better understand the fundamental properties of matter and the universe. Simulating a single nucleus in a neutron star crust using the Compressible Liquid Drop Model, we can calculate how the composition of the nucleus changes as it sinks into the crust through three potential nuclear reactions: electron capture, neutron emission, and pycnonuclear fission. Determining which nuclear reactions occur in a neutron star crust involves calculating reaction rates, comparing them under varying local conditions, and assessing the most energetically favorable reaction, considering factors such as temperature, density, and energy output. These reactions become more prominent as the density increases, causing the nuclei to become more compact as the WS-Cell moves deeper into the neutron star's crust. This framework allows us to test specific parameters of nuclear interactions within the neutron star, particularly focusing on the surface strength of nuclei and the description of the nuclear forces' called Skyrme, specifically the parameter proportional to internal pressure. By tracking the energy-efficient route and assessing the simulation's realism, we can calculate and compare the energy produced by these nuclear reactions. Future methods will involve calculating the total energy against pressure, noting that pressure variations are less significant as you delve deeper into the inner crust compared to density fluctuations. Additionally, we will compute the heat output from these nuclear reactions, which is crucial for future research on neutron star crust cooling.